scholarly journals Exploring star formation in high-mass galaxies in the low-z universe

2018 ◽  
Author(s):  
◽  
James Runge
Keyword(s):  
Star Formation ◽  
Galaxy Evolution ◽  
Star Formation Rate ◽  
Formation Rate ◽  
Value Added ◽  
Sloan Digital Sky Survey ◽  
High Mass ◽  
Wide Field ◽  
Max Planck ◽  
Field Sample

We present a quantitative analysis of high-mass, low-z galaxies in order to investigate the 'downsizing' scenario of galaxy evolution. High-mass, low-z galaxies with ongoing star formation, antithetical to the 'downsizing' model, are identified using the 22�m data (W4 band) from the Wide-field Infrared Survey Explorer (WISE). A cluster and field sample is chosen to investigate any possible environmental effects. The cluster sample is based upon the GMBCG catalog, which contains 55,424 brightest cluster galaxies (BCGs) at 0.1 [less than or about] z [less than or about] 0.55 identified in the Sloan Digital Sky Survey (SDSS). We identify 389 W4-detected BCGs (W4BCGs) that have median SFRs of [about]50 M[symbol]/yr based upon their total IR luminosity (LIR), which is attributed to dust-enshrouded star formation. BCGs with such high SFRs are found in "cool-core" clusters and the star formation is thought to be fueled by a "cooling flow." Using Chandra X-ray data, it is shown that a subset of BCGs do reside within coolcores, but their mass deposition rates cannot account for the SFR. For comparison, a field sample is drawn from the Max-Planck Institute for Astrophysics - John Hopkins University (MPA-JHU) "value-added" SDSS DR7 catalog of spectrum measurements. A set of 1,244 high-mass, elliptical field galaxies within the same redshift range as the W4BCG catalog are identified for comparison. The median mass for the field sample is lower than the W4BCGs (Log(M/M[symbol])=10.9 and 11.2 respectively), as are their SFRs. However, the specific star formation rate (sSFR), the star formation rate per stellar mass, is comparable for both groups (Log(sSFR)[about]-9.7). This possibly reveals that there is no environmental dependence on the sSFR for these W4-detected galaxies. While a possible mechanism responsible for the SFR was identified for the W4BCGs, the process responsible for the star formation in the field sample requires further investigation.

scholarly journals Using u band emission to trace star formation rates of galaxies

2016 ◽  
Vol 12 (S323) ◽  
pp. 392-393
Author(s):  
Zhimin Zhou
Keyword(s):  
Star Formation ◽  
Star Formation Rate ◽  
Formation Rate ◽  
Sloan Digital Sky Survey ◽  
Wide Field ◽  
The South ◽  
Evolution Of Galaxies ◽  
Band Emission ◽  
Sky Survey ◽  
Infrared Survey

AbstractStar formation rate (SFR) is one of the most important diagnostics in understanding the evolution of galaxies across cosmic times. In order to explore the possibility of using the optical u-band luminosities to estimate SFRs of galaxies, we show the correlations between u band, Hα and infrared luminosities by combing the data from the South Galactic Cap u band Sky Survey (SCUSS) with the Sloan Digital Sky Survey (SDSS) and the Wide-field Infrared Survey Explorer (WISE). We derive the u versus Hα relation and the u and 12 μm relations to calibrate the u-band luminosity as an SFR indicator.

scholarly journals A WIDE-FIELD HIGH-RESOLUTION H I MOSAIC OF MESSIER 31. I. OPAQUE ATOMIC GAS AND STAR FORMATION RATE DENSITY

2009 ◽  
Vol 695 (2) ◽  
pp. 937-953 ◽  
Author(s):  
R. Braun ◽  
D. A. Thilker ◽  
R. A. M. Walterbos ◽  
E. Corbelli
Keyword(s):  
Star Formation ◽  
High Resolution ◽  
Star Formation Rate ◽  
Formation Rate ◽  
Wide Field ◽  
Atomic Gas

scholarly journals Feedback by supermassive black holes in galaxy evolution: impacts of accretion and outflows on the star formation rate

2019 ◽  
Vol 486 (2) ◽  
pp. 1509-1522 ◽  
Author(s):  
Mojtaba Raouf ◽  
Joseph Silk ◽  
Stanislav S Shabala ◽  
Gary A Mamon ◽  
Darren J Croton ◽  
...  
Keyword(s):  
Black Holes ◽  
Star Formation ◽  
Galaxy Evolution ◽  
Star Formation Rate ◽  
Formation Rate ◽  
Supermassive Black Holes

scholarly journals Star Formation Rate Indicators in Wide-Field Infrared Survey Preliminary Release

2012 ◽  
Vol 33 (2) ◽  
pp. 213-220 ◽  
Author(s):  
Fei Shi ◽  
Xu Kong ◽  
James Wicker ◽  
Yang Chen ◽  
Zi-Qiang Gong ◽  
...  
Keyword(s):  
Star Formation ◽  
Star Formation Rate ◽  
Formation Rate ◽  
Wide Field ◽  
Infrared Survey

scholarly journals A Photometric Survey of Field Stars in the Large Magellanic Cloud: Probing its Star-Formation History

1999 ◽  
Vol 190 ◽  
pp. 343-344 ◽  
Author(s):  
T. A. Smecker-Hane ◽  
J. S. Gallagher ◽  
Andrew Cole ◽  
P. B. Stetson ◽  
E. Tolstoy
Keyword(s):  
Star Formation ◽  
Galaxy Evolution ◽  
Stellar Population ◽  
Formation Rate ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Star Formation History ◽  
Wide Field ◽  
Formation History ◽  
Magnitude Diagram

The Large Magellanic Cloud (LMC) is unique among galaxies in the Local Group in that it is the most massive non-spiral, is relatively gas-rich, and is actively forming stars. Determining its star-formation rate (SFR) as a function of time will be a cornerstone in our understanding of galaxy evolution. The best method of deriving a galaxy's past SFR is to compare the densities of stars in a color-magnitude diagram (CMD), a Hess diagram, with model Hess diagrams. The LMC has a complex stellar population with ages ranging from 0 to ~ 14 Gyr and metallicities from −2 ≲ [Fe/H] ≲ −0.4, and deriving its SFR and simultaneously constraining model input parameters (distance, age-metallicity relation, reddening, and stellar models) requires well-populated CMDs that span the magnitude range 15 ≤ V ≤ 24. Although existing CMDs of field stars in the LMC show tantalizing evidence for a significant burst of star formation that occurred ~ 3 Gyr ago (for examples, see Westerlund et al. 1995; Vallenari et al. 1996; Elson, et al. 1997; Gallagher et al. 1999, and references therein), estimates of the enhancement in the SFR vary from factors of 3 to 50. This uncertainty is caused by the relatively large photometric errors that plague crowded ground-based images, and the small number statistics that plague CMDs created from single Wide Field Planetary Camera 2 (WFPC2) images.

scholarly journals Properties of simulated galaxies and supermassive black holes in cosmic voids

2020 ◽  
Vol 493 (1) ◽  
pp. 899-921
Author(s):  
Mélanie Habouzit ◽  
Alice Pisani ◽  
Andy Goulding ◽  
Yohan Dubois ◽  
Rachel S Somerville ◽  
...  
Keyword(s):  
Black Holes ◽  
Star Formation ◽  
Star Formation Rate ◽  
Large Fraction ◽  
Formation Rate ◽  
Dark Matter Halo ◽  
Wide Field ◽  
Void Galaxies ◽  
Low Mass ◽  
Cosmic Voids

ABSTRACT Cosmic voids, the underdense regions of the cosmic web, are widely used to constrain cosmology. Voids contain few, isolated galaxies, presumably expected to be less evolved and preserving memory of the pristine Universe. We use the cosmological hydrodynamical simulation Horizon-AGN coupled to the void finder vide to investigate properties of galaxies in voids at z = 0. We find that, closer to void centres, low-mass galaxies are more common than their massive counterparts. At a fixed dark matter halo mass, they have smaller stellar masses than in denser regions. The star formation rate of void galaxies diminishes when approaching void centres, but their specific star formation rate slightly increases, suggesting that void galaxies form stars more efficiently with respect to their stellar mass. We find that this cannot only be attributed to the prevalence of low-mass galaxies. The inner region of voids also predominantly hosts low-mass black holes (BHs). However, the BH mass-to-galaxy mass ratios resemble those of the whole simulation at z = 0. Our results suggest that even if the growth channels in cosmic voids are different from those in denser environments, voids grow their galaxies and BHs in a similar way. While a large fraction of the BHs have low Eddington ratios, we find that $\text{$\sim$} 20{{\ \rm per\ cent}}$ could be observed as active galactic nuclei with $\log _{10} L_{\rm 2\!-\!10 \, keV}=41.5\!-\!42.5 \, \rm erg\, s^{-1}$. These results pave the way to future work with larger next-generation hydro-simulations, aiming to confirm our findings and prepare the application on data from upcoming large surveys such as Prime Focus Spectrograph, Euclid, and Wide Field Infrared Survey Telescope.

scholarly journals 2–10 keV luminosity of high-mass binaries as a gauge of ongoing star-formation rate

2004 ◽  
Vol 419 (3) ◽  
pp. 849-862 ◽  
Author(s):  
M. Persic ◽  
Y. Rephaeli ◽  
V. Braito ◽  
M. Cappi ◽  
R. Della Ceca ◽  
...  
Keyword(s):  
Star Formation ◽  
Star Formation Rate ◽  
Formation Rate ◽  
High Mass

scholarly journals A correlation between star formation rate and average black hole accretion rate in star forming galaxies

2013 ◽  
Vol 9 (S304) ◽  
pp. 302-306
Author(s):  
Chien-Ting J. Chen ◽  
Ryan C. Hickox
Keyword(s):  
Star Formation ◽  
Galaxy Evolution ◽  
Star Formation Rate ◽  
Accretion Rate ◽  
Formation Rate ◽  
Far Infrared ◽  
Host Galaxies ◽  
Star Forming ◽  
Black Hole Accretion ◽  
Strong Linear Correlation

AbstractWe present the results of recent studies on the co-evolution of galaxies and the supermassive black holes (SMBHs) using Herschel far-infrared and Chandra X-ray observations in the Boötes survey region. For a sample of star-forming (SF) galaxies, we find a strong correlation between galactic star formation rate and the average SMBH accretion rate in SF galaxies. Recent studies have shown that star formation and AGN accretion are only weakly correlated for individual AGN, but this may be due to the short variability timescale of AGN relative to star formation. Averaging over the full AGN population yields a strong linear correlation between accretion and star formation, consistent with a simple picture in which the growth of SMBHs and their host galaxies are closely linked over galaxy evolution time scales.

scholarly journals Star Formation Rate Indicators in the Sloan Digital Sky Survey

2003 ◽  
Vol 599 (2) ◽  
pp. 971-991 ◽  
Author(s):  
A. M. Hopkins ◽  
C. J. Miller ◽  
R. C. Nichol ◽  
A. J. Connolly ◽  
M. Bernardi ◽  
...  
Keyword(s):  
Star Formation ◽  
Star Formation Rate ◽  
Formation Rate ◽  
Sloan Digital Sky Survey ◽  
Sky Survey

Bar effects on ionized gas properties and dust content in galaxy centers

2014 ◽  
Vol 10 (S309) ◽  
pp. 356-356
Author(s):  
A. Zurita ◽  
E. Florido ◽  
I. Pérez ◽  
P. Coelho ◽  
D. A. Gadotti
Keyword(s):  
Star Formation ◽  
Galaxy Evolution ◽  
Observational Studies ◽  
Star Formation Rate ◽  
Unit Area ◽  
Formation Rate ◽  
Line Ratio ◽  
Ionized Gas ◽  
Bulge Formation ◽  
Gas Properties

AbstractObservations and simulations indicate that bars are important agents to transfer material towards galaxy centers. However, observational studies devoted to investigate the effects of bars in galaxy centers are not yet conclusive. We have used a sample (Coelho & Gadotti 2011) of nearby face–on galaxies with available spectra (SDSS database) to investigate the footprints of bars in galaxy centers by analysing the central ionized gas properties of barred and unbarred galaxies separately. We find statistically significant differences in the Hβ Balmer extinction, star formation rate per unit area, in the [S ii]λ6717/[S ii]λ6731 line ratio, and notably in the N2 parameter (N2 = log([N ii]λ6583/Hα)). A deeper analysis reflects that these differences are only relevant for the less massive bulges (≲1010M⊙). These results have important consequences for studies on bulge formation and galaxy evolution.

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